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The Magnetic Field in the Solar Atmosphere [PDF]
Astronomy and Astrophysics Review, 2014 This publication provides an overview of magnetic fields in the solar atmosphere with the focus lying on the corona. The solar magnetic field couples the solar interior with the visible surface of the Sun and with its atmosphere. It is also responsible for all solar activity in its numerous manifestations.
Thomas Wiegelmann +2 more
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Space Science Reviews, 1964
This paper is a review of our observational knowledge on solar magnetic fields. In Section 1 we make an attempt to summarize all observations of the general magnetic field (m.f.) of the Sun. Section 2 deals with the local m.f. at low latitudes and their connection with some features on the disk. The m.f.
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This paper is a review of our observational knowledge on solar magnetic fields. In Section 1 we make an attempt to summarize all observations of the general magnetic field (m.f.) of the Sun. Section 2 deals with the local m.f. at low latitudes and their connection with some features on the disk. The m.f.
exaly +2 more sources
Magnetic fields in the solar photosphere
Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences, 2008Recent high-resolution observations of the surface of the Sun have revealed the fine structure of a vast array of complex photospheric magnetic features. Observations of these magnetic field structures have already greatly enhanced our theoretical understanding of the interactions between magnetic fields and turbulent convection, and future ...
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Intermittency of the Solar Magnetic Field and Solar Magnetic Activity Cycle
Solar Physics, 2017Small-scale solar magnetic fields demonstrate features of fractal intermittent behavior, which requires quantification. For this purpose we investigate how the observational estimate of the solar magnetic flux density \(B\) depends on resolution \(D\) in order to obtain the scaling \(\ln B_{D} = - k \ln D +a\) in a reasonably wide range. The quantity \(
A. S. Shibalova +2 more
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1966
Abstract : A study was conducted of the correspondence of photospheric magnetic fields with structures and transient phenomena observed in the chromosphere. The primary data used were isogauss maps constructed from the Mt. Wilson daily, full disk magnetograms for the period 1959 through 1962, and three fine-scan magnetograms made on 6 July 1965.
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Abstract : A study was conducted of the correspondence of photospheric magnetic fields with structures and transient phenomena observed in the chromosphere. The primary data used were isogauss maps constructed from the Mt. Wilson daily, full disk magnetograms for the period 1959 through 1962, and three fine-scan magnetograms made on 6 July 1965.
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Magnetic field of the solar wind
Solar Physics, 1976Relationship between the geoefficiency of the solar flares as well as of the active regions passing the central meridian of the Sun and the configuration of the large scale solar magnetic field is studied. It is shown that if the tangential component of the large scale magnetic field at the active region or at the flare region is directed southwards ...
M.I. Pudovkin, A.D. Chertkov
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2003
The proximity of the Sun allows us to make detailed measurements on the properties of solar magnetic fields. The long term systematic changes in the solar magnetic field pattern indicate a global origin. A global dynamo can be sustained by the interaction of solar convection with solar rotation.
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The proximity of the Sun allows us to make detailed measurements on the properties of solar magnetic fields. The long term systematic changes in the solar magnetic field pattern indicate a global origin. A global dynamo can be sustained by the interaction of solar convection with solar rotation.
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Elements and Patterns in the Solar Magnetic Field
Annual Review of Astronomy and Astrophysics, 1987and the non thermal processes in th e solar atmosphere indicate the importance of mag netic fields in turbulent cosmical bodies. We are now aware that magnetic processes also occur in other stars, in protostars, in supernova remnants, in gaseous disks of galaxies, in accretion disks around compact stars, and in active nuclei of galaxies.
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The Solar Magnetic Field and the Solar Activity
1965The Sun has a mass of 2 × 1033 g, a radius of 7 × 1010 cm, a luminosity of 3.6 × 1033 ergs sec-1. The internal structure of the Sun is determined by the equation of hydrostatic equilibrium, the equation of transfer of energy and the equation of energy generation by thermonuclear reactions.
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